Many observational studies of the solar corona at low frequencies have measured observed source sizes. Work done by [1]} and [2]} resolved sources of 30-–40 using the Very Large Array [3]}, [4]} between 328–333MHz. A sub-arcminute structure associated with a Type I noise storm was observed by [5]} at 169 MHz using the Nançay Radioheliograph [6]} and by [7]}, [8]} at 236 MHz and 327 MHz using the NRH and the Giant Meterwave Radio Telescope [9]} in tandem. At lower frequencies, [10]} observed sources of approximately 3 at 34.5 MHz using the Decameter Wave Radio Telescope in the Gauribidanur Observatory [11]}. However, due to insufficient baselines lengths, none of the above studies have imaged sub-arcsecond structure in the metric and decimetric regime, despite X-ray and extreme ultraviolet (EUV) imaging showing the corona to be highly structured on arcsecond and sub-arcsecond scales [12]}, [13]}, [14]}.
